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The kinematics and distribution of classical Cepheids within ∼3 kpc from the Sun suggest the existence of the outer ring  R  1  R  ′ 2  in the Galaxy. The optimum value of the solar position angle with respect to the major axis of the bar,  θ  b , providing the best agreement between the distribution of Cepheids and model particles, is  θ  b  = 37° ±13°. The kinematical features obtained for Cepheids with negative galactocentric radial velocity  V  R  are consistent with the solar location near the descending segment of the outer ring  R  2 . The sharp rise of extinction toward of the Galactic center can be explained by the presence of the outer ring  R  1  near the Sun. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)

Classical Cepheids in the Galactic outer ring R 1 R ′ 2